准平衡态的中子星
Binary Neutron Stars in Quasi-equilibrium
摘要：
在广义相对论的各种状态方程下，构造了中子星双星的准平衡序列。在Isenberg-Wilson-Mathews近似下的Einstein约束方程与流体定常平衡的相对论方程在无旋流动假设下一起求解。我们专注于不等质量序列以及等质量序列，并比较这些结果。我们研究了准平衡序列、序列终点、轨道角速度随时间的变化，以及质量比、双星系统的总质量和中子星的状态方程的变化。发现质量脱落极限下的轨道角速度可以由解析估算得到的经验公式确定。我们还提供了160个序列的表格，这将是有用的指导方针，数值模拟的螺旋和合并在不久的将来进行。
英文摘要：
Quasi-equilibrium sequences of binary neutron stars are constructed for a variety of equations of state in general relativity. Einstein's constraint equations in the Isenberg-Wilson-Mathews approximation are solved together with the relativistic equations of hydrostationary equilibrium under the assumption of irrotational flow. We focus on unequal-mass sequences as well as equal-mass sequences, and compare those results. We investigate the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It is found that the orbital angular velocity at the mass-shedding limit can be determined by an empirical formula derived from an analytic estimation. We also provide tables for 160 sequences which will be useful as a guideline of numerical simulations for the inspiral and merger performed in the near future.
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